Galactic chemical evolution

Hydrogen through zinc

Francis Timmes, S. E. Woosley, Thomas A. Weaver

Research output: Contribution to journalArticle

746 Citations (Scopus)

Abstract

Using the output from a grid of 60 Type II supernova models (Woosley & Weaver 1995) of varying mass (11 ≲ M/M ≲ 40) and metallicity (0, 10-4, 0.01, 0.1, and 1 Z), the chemical evolution of 76 stable isotopes, from hydrogen to zinc, is calculated. The chemical evolution calculation employs a simple dynamical model for the Galaxy (infall with a 4 Gyr e-folding timescale onto an exponential disk and 1/r2 bulge), and standard evolution parameters, such as a Salpeter initial mass function and a quadratic Schmidt star formation rate. The theoretical results are compared in detail with observed stellar abundances in stars with metallicities in the range -3.0 ≲ [Fe/H] ≲ 0.0 dex. While our discussion focuses on the solar neighborhood where there are the most observations, the supernova rates, an intrinsically Galactic quantity, are also discussed. Sampling 4.6 Gyr ago at a distance of 8.5 kpc, we find a composition at the solar circle that is in excellent agreement with the solar abundances from hydrogen to zinc. Type Ia supernovae provide about one-third of solar iron abundance in this distribution. Oxygen comes from the massive stars, but carbon and nitrogen come chiefly from stars with M ≲ 8 M. The light metal and iron group elements, with the exception of titanium, are in generally good agreement with the stellar abundance data. We also find an age-metallicity relation, a G dwarf distribution, and present-day supernova rates that are in satisfactory agreement with observations. The neutrino process provides a good explanation for the origin of 11B and 19F and the increase in 7Li over its canonical homogeneous big bang value. In order to explain the observed helium-to-metal enrichment (ΔY/ΔZ ≃ 4), we find a favored cutoff in the mass of supernovae that eject all material external to the iron core of about 30 M, but this limit may be increased by considering the effects of mass loss. The robustness of the results to variations in the iron yields of the Type II supernova models are examined.

Original languageEnglish (US)
Pages (from-to)617-658
Number of pages42
JournalAstrophysical Journal, Supplement Series
Volume98
Issue number2
StatePublished - Jun 1995
Externally publishedYes

Fingerprint

chemical evolution
galactic evolution
supernovae
zinc
hydrogen
iron
metallicity
metal
helium
titanium
folding
stars
stable isotope
solar neighborhood
star formation rate
timescale
massive stars
metals
oxygen
chemical

Keywords

  • Galaxy: abundances
  • Galaxy: evolution
  • Galaxy: stellar content
  • Nuclear reactions, nucleosynthesis, abundances

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Galactic chemical evolution : Hydrogen through zinc. / Timmes, Francis; Woosley, S. E.; Weaver, Thomas A.

In: Astrophysical Journal, Supplement Series, Vol. 98, No. 2, 06.1995, p. 617-658.

Research output: Contribution to journalArticle

Timmes, F, Woosley, SE & Weaver, TA 1995, 'Galactic chemical evolution: Hydrogen through zinc', Astrophysical Journal, Supplement Series, vol. 98, no. 2, pp. 617-658.
Timmes, Francis ; Woosley, S. E. ; Weaver, Thomas A. / Galactic chemical evolution : Hydrogen through zinc. In: Astrophysical Journal, Supplement Series. 1995 ; Vol. 98, No. 2. pp. 617-658.
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